Bibcode
Wünsch, Richard; Palouš, Jan; Tenorio-Tagle, Guillermo; Muñoz-Tuñón, C.; Ehlerová, Soňa
Referencia bibliográfica
Formation, evolution, and survival of massive star clusters, Proceedings of the International Astronomical Union, IAU Symposium, Volume 316, pp. 294-301
Fecha de publicación:
3
2017
Número de citas
2
Número de citas referidas
2
Descripción
Massive stars in young massive clusters insert tremendous amounts of
mass and energy into their surroundings in the form of stellar winds and
supernova ejecta. Mutual shock-shock collisions lead to formation of hot
gas, filling the volume of the cluster. The pressure of this gas then
drives a powerful cluster wind. However, it has been shown that if the
cluster is massive and dense enough, it can evolve in the so-called
bimodal regime, in which the hot gas inside the cluster becomes
thermally unstable and forms dense clumps which are trapped inside the
cluster by its gravity. We will review works on the bimodal regime and
discuss the implications for the formation of subsequent stellar
generations. The mass accumulates inside the cluster and as soon as a
high enough column density is reached, the interior of the clumps
becomes self-shielded against the ionising radiation of stars and the
clumps collapse and form new stars. The second stellar generation will
be enriched by products of stellar evolution from the first generation,
and will be concentrated near the cluster center.